Journal Article

Relativistic hybrid stars with super-strong toroidal magnetic fields: an evolutionary track with QCD phase transition

Nobutoshi Yasutake, Kenta Kiuchi and Kei Kotake

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 401, issue 3, pages 2101-2112
Published in print January 2010 | ISSN: 0035-8711
Published online January 2010 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2009.15813.x
Relativistic hybrid stars with super-strong toroidal magnetic fields: an evolutionary track with QCD phase transition

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We investigate the structures of hybrid stars, which feature a quark core surrounded by a hadronic matter mantle, with super-strong toroidal magnetic fields in full general relativity. Modelling the equation of state (EOS) with a first-order transition by bridging the MIT bag model for the description of quark matter and the nuclear EOS by Shen et al., we numerically construct thousands of equilibrium configurations for studying the effects of phase transition. It is found that the appearance of the quark phase can affect the distributions of the magnetic fields inside the hybrid stars, making the maximum field strength up to about 30 per cent larger than for the normal neutron stars. Using the equilibrium configurations, we explore the possible evolutionary paths to the formation of hybrid stars due to the spin-down of magnetized rotating neutron stars. We find that the energy released by the phase transition to the hybrid stars is quite large (≲1052 erg) even for super-strongly magnetized compact stars. Our results suggest that the strong gravitational-wave emission and the sudden spin-up signature could be observable signals of the quantum chromodynamics phase transition, possibly for a source out to megaparsec distances.

Keywords: dense matter; equation of state; gravitation; stars: neutron; stars: rotation

Journal Article.  7939 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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